用于天文观测台设计和建模的混合传播物理学:以日冕仪为例

Jaren Ashcraft, Ewan S Douglas, Daewook Kim, A. Riggs
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引用次数: 0

摘要

摘要对于衍射受限的光学系统,准确的物理光学模型是正确评估仪器性能的必要条件。天文观测台配备的日冕仪用于系外行星的直接成像,需要物理光学模型来模拟偏差和衍射的影响。准确了解天文台的点扩散函数(PSF)对于设计高对比度成像仪器和模拟天体物理观测是不可或缺的。目前的技术水平是在多个软件包中建立错位、射线像差和衍射模型,这使得设计过程变得复杂。高斯小波束分解(GBD)是一种基于射线的衍射计算方法,已广泛应用于商业光学设计软件中。通过利用天文台射线模型的数据进行相干计算,射线像差误差可以直接输入日冕仪的物理光学模型,使天文台模型更加综合。我们开发了 GBD 转移矩阵法的正式算法,并将其与分析结果和传统物理光学模型进行对比评估,以评估 GBD 是否适用于高对比度成像模拟。我们对天文台 PSF 的 GBD 模拟与分析 Airy 函数相比,其总和归一化均方根差值≈10 - 6。然后通过系外行星成像日冕仪的弗劳恩霍夫模型传播这些场,其平均残余数值对比度为 4 × 10 - 11,内工作角附近的最大值为 5 × 10 - 9。这些结果表明,GBD 作为高对比度成像中一种可行的传播技术,在未来的发展中大有可为。我们在一个开源软件包中开发了这一算法,并概述了其继续发展的路径,以提高使用 GBD 进行衍射模拟的准确性和灵活性。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
Hybrid propagation physics for the design and modeling of astronomical observatories: a coronagraphic example
Abstract. For diffraction-limited optical systems, an accurate physical optics model is necessary to properly evaluate instrument performance. Astronomical observatories outfitted with coronagraphs for direct exoplanet imaging require physical optics models to simulate the effects of misalignment and diffraction. Accurate knowledge of the observatory’s point-spread function (PSF) is integral for the design of high-contrast imaging instruments and simulation of astrophysical observations. The state of the art is to model the misalignment, ray aberration, and diffraction across multiple software packages, which complicates the design process. Gaussian beamlet decomposition (GBD) is a ray-based method of diffraction calculation that has been widely implemented in commercial optical design software. By performing the coherent calculation with data from the ray model of the observatory, the ray aberration errors can be fed directly into the physical optics model of the coronagraph, enabling a more integrated model of the observatory. We develop a formal algorithm for the transfer-matrix method of GBD and evaluate it against analytical results and a traditional physical optics model to assess the suitability of GBD for high-contrast imaging simulations. Our GBD simulations of the observatory PSF, when compared to the analytical Airy function, have a sum-normalized RMS difference of ≈10  −  6. These fields are then propagated through a Fraunhofer model of an exoplanet imaging coronagraph where the mean residual numerical contrast is 4  ×  10  −  11, with a maximum near the inner working angle at 5  ×  10  −  9. These results show considerable promise for the future development of GBD as a viable propagation technique in high-contrast imaging. We developed this algorithm in an open-source software package and outlined a path for its continued development to increase the accuracy and flexibility of diffraction simulations using GBD.
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